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Erratum
This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201116631]


Table 1

Observational and derived line parameters.

N2H+ (3–2) N2D+ (2–1)


Source VLSR FWHM τ Tex VLSR FWHM N(N2H+) N(N2D+) Dfrac Tk††
(K km s-1) (km s-1) (km s-1) (K) (K km s-1) (km s-1) (km s-1) (× 1013 cm-2) (× 1012 cm-2) (K)

HMSCs I00117-MM2 2.9(0.1) –35.51(0.01) 2.27(0.04) <0.1 7a 0.48(0.02) –35(1) 1.65(0.7) 3.1(0.3) 10(1) 0.32(0.06) 14h
AFGL5142-EC 20.7(0.1) –2.21(0.01) 3.42(0.01) 0.51(0.01) 44.1(0.1)b 0.48(0.03) –2.73(0.04) 1.35(0.1) 4.8(0.5) 3.8(0.6) 0.08(0.01) 25h
05358-mm3 43.0(0.1) –15.34(0.01) 2.200(0.003) 5(2) 34(4)b 0.16(0.02) –15.5(0.2) 2.9(0.4) 9.3(0.9) 1.1(0.3) 0.012(0.003) 30h
G034-G2(MM2) 2.0(0.1) 42.2(0.02) 1.950(0.003) 1.51(0.01) 7.57(0.03)b 0.76(0.03) 41.80(0.08) 1.6(0.3) 1.7(0.2) 13(2) 0.7(0.2) − −
G034-F2(MM7) 1.65(0.05) 58.3(0.1) 2.84(0.3) <0.1 16c 0.25(0.03) 57.7(0.2) 1.4(0.9) 0.42(0.04) 1.8(0.3) 0.43(0.09)
G034-F1(MM8) 1.08(0.08) 58.1(0.2) 2.5(0.5) 16c 0.17(0.03) 57(4) 2.0(1.5) 0.28(0.03) 1.2(0.3) 0.4(0.1)
G028-C1(MM9) 2.4(0.1) 80.32(0.03) 2.4(0.2) 3(1) 6.4(0.4)b 0.50(0.03) 80.10(0.08) 2.6(0.3) 3.4(0.3) 13(2) 0.38(0.07) 17i
I20293-WC 9.4(0.1) 7.490(0.008) 3.560(0.003) <0.1 8.5a 0.82(0.03) 7.3(0.3) 1.0(0.9) 5.9(0.6) 11(2) 0.19(0.3) 17h
I22134-G 6.9(0.1) –18.20(0.01) 1.01(0.02) 3.3(0.2) 15.9(0.3)b 0.06(0.01) –19.7(0.2) 0.8(0.5) 1.8(0.2) 0.4(0.2) 0.023(0.009) 25h
I22134-B 2.4(0.1) –18.3(0.04) 0.83(0.03) 2.3(0.3) 10.4(0.4)b 0.09(0.02) –18.8(0.06) 0.5(0.4) 1.0(0.1) 0.9(0.2) 0.09(0.02) 17h

HMPOs I00117-MM1 5.5(0.1) –35.89(0.01) 1.50(0.04) 2.4(0.3) 19.3(0.4)b ≤0.07 1.26(0.1) ≤0.5 ≤0.04 20h
I04579-VLA1††† 1.23(0.02) –17.51(0.06) 1.8(0.2) <0.1 74d ≤0.14 0.4(0.05) ≤1.5 ≤0.4 74j
AFGL5142-MM 27.2(0.1) –2.470(0.004) 2.820(0.006) 3.4(0.1) 39.24(0.01)b 0.40(0.02) –2.7(0.1) 2.3(0.3) 6.1(0.6) 3.0(0.5) 0.049(0.009) 34h
05358-mm1 30.3(0.1) –15.588(0.003) 2.040(0.003) 5(1) 46(2)b 0.15(0.02) –15.7(0.3) 2.5(0.6) 7.2(0.7) 1.2(0.2) 0.017(0.004) 39h
18089–1732 31.4(0.2) 32.40(0.004) 4.960(0.001) <0.1 38d 0.29(0.03) 33.3(0.6) 3(1) 7.0(0.7) 2.2(0.3) 0.031(0.006) 38k
18517+0437 19.2(0.1) 44.44(0.03) 3.08(0.01) <0.1 47e 0.15(0.02) 44.2(0.5) 3(1) 4.6(0.5) 1.2(0.2) 0.026(0.006)
G75-core 6.5(0.1) 0.01(0.02) 3.99(0.04) <0.1 96d ≤ 0.05 2.4(0.2) ≤0.69 ≤0.029 96h
I20293-MM1 29.6(0.1) 6.69(0.02) 1.610(0.002) 6.4(0.1) 50.1(0.1)b 0.64(0.03) 5.69(0.08) 1.8(0.3) 7.3(0.7) 5.4(0.8) 0.07(0.01) 37h
I21307 6.5(0.1) –46.29(0.02) 2.98(0.05) <0.1 21d ≤ 0.06 1.5(0.1) ≤0.4 ≤0.03 21j
I23385 9.41(0.08) –49.88(0.01) 3.02(0.03) <0.1 37d 0.08(0.05) –48(3) 1.2(0.9) 2.1(0.2) 0.6(0.1) 0.028(0.009) 37l

UC HII G5.89–0.39 84.1(0.3) 9.180(0.003) 5.900(0.009) <0.1 20 f 0.50(0.03) 7.6(0.1) 1.5(0.3) 19(2) 3.4(0.5) 0.018(0.003)
I19035-VLA1 13.7(0.2) 32.62(0.01) 4.49(0.03) <0.1 19.0(0.2)g 0.18(0.03) 32.5(0.1) 1.4(0.3) 3.2(0.3) 1.3(0.3) 0.04(0.01) 39h
19410+2336 33.3(0.1) 22.90(0.005) 3.550(0.001) <0.1 21d 0.52(0.05) 22.5(0.08) 1.5(0.3) 7.4(0.7) 3.5(0.5) 0.047(0.009) 21k
ON1 30.9(0.2) 12.579(0.001) 4.340(0.001) <0.1 26d 0.17(0.05) 11.7(0.9) 3.13(1.65) 6.6(0.7) 1.1(0.2) 0.017(0.004) 26m
I22134-VLA1 2.5(0.08) –18.11(0.01) 1.30(0.06) 1.9(0.4) 10.6(0.5)b 0.08(0.01) –19.2(0.4) 0.7(1.0) 1.0(0.1) 0.8(0.2) 0.08(0.02) 47h
23033+5951 19.6(0.1) –52.72(0.03) 3.530(0.002) <0.1 25d 0.52(0.02) –53.2(0.5) 0.8(0.5) 4.4(0.4) 3.5(0.5) 0.08(0.02) 25k
NGC7538-IRS9 13.9(0.1) –56.814(0.006) 3.42(0.03) <0.1 20f 0.14(0.02) –57(2) 2.6(0.5) 3.2(0.3) 0.9(0.2) 0.030(0.008)

Notes. Columns 2–6 list integrated intensity over all the hyperfine components (), peak velocity (VLSR), full width at half maximum (FWHM) corrected for hyperfine splitting, opacity (τ) and excitation temperature (Tex), from N2H+ (3–2); Cols. 7–9 list , VLSR and FWHM for the N2D+ (2–1) lines. In Cols. 10 and 11 we give the N2H+ and N2D+ column densities, respectively, and their ratio (Dfrac) is given in Col. 12. Column 13 shows the kinetic temperature (Tk) measured from ammonia observations. Uncertainties are given in parentheses.

(†)

Tex associated with uncertainties are calculated from the data, the others are assumed as explained in the footnotes;

(††)

Tk are derived from ammonia rotation temperatures following Tafalla et al. (2004);

(a)

Tex ~ 1/2 Tk, based on the results derived in this work for the HMSCs with well constrained Tex and Tk, except the “warm” ones;

(b)

derived from the (3–2) line parameters obtained from the hyperfine fitting procedure and corrected for filling factor (see also the CLASS User Manual (http://iram.fr/IRAMFR/GILDAS/doc/html/class-html/class.html));

(c)

average value for HMSCs;

(d)

Tex~ Tk, based on the results derived in this work for the HMPOs with well constrained Tex and Tk, and on the findings of Fontani et al. (2006) towards a sample of massive cores containing both HMPOs and UC HII regions;

(e)

average value for HMPOs;

(f)

average value for UCHIIs;

(g)

computed from the N2H+ (1–0) line;

(h)

from VLA observations (Busquet 2010; Sánchez-Monge 2011; Palau, priv. comm.);

(i)

from Effelsberg observations (Pillai et al. 2006);

(j)

from Effelsberg observations (Molinari et al. 1996);

(k)

from Effelsberg observations (Sridharan et al. 2002);

(l)

from VLA observations (Fontani et al. 2004);

(m)

from Effelsberg observations (Jijina et al. 1999);

(†††)

N2H+ parameters are derived from the (1–0) line, for which is the integrated intensity of the isolated component (F1F = 1,0–1, 1) appropriately normalised and assumed to be optically thin. However, because observations were obtained under very bad weather conditions, the Dfrac upper limit derived from this source is unreliable and we decided to exclude it in the following analysis.

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